Primordial Black Hole Microlensing: The Einstein Crossing Time Distribution. (arXiv:1904.01771v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lu_J/0/1/0/all/0/1">Jessica R. Lu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lam_C/0/1/0/all/0/1">Casey Y. Lam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Medford_M/0/1/0/all/0/1">Michael Medford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dawson_W/0/1/0/all/0/1">William Dawson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golovich_N/0/1/0/all/0/1">Nathan Golovich</a>

Gravitational microlensing is one of the few means of finding primordial
black holes (PBHs), if they exist. Recent LIGO detections of 30 Msun black
holes have re-invigorated the search for PBHs in the 10-100 Msun mass regime.
Unfortunately, individual PBH microlensing events cannot easily be
distinguished from stellar lensing events from photometry alone. However, the
distribution of microlensing timescales (tE, the Einstein radius crossing time)
can be analyzed in a statistical sense using models of the Milky Way with and
without PBHs. While previous works have presented both theoretical models and
observational constrains for PBHs (e.g. Calcino et al. 2018; Niikura et al.
2019), surprisingly, they rarely show the observed quantity — the tE
distribution — for different abundances of PBHs relative to the total dark
matter mass (fPBH). We present a simple calculation of how the tE distribution
changes between models with and without PBHs.

Gravitational microlensing is one of the few means of finding primordial
black holes (PBHs), if they exist. Recent LIGO detections of 30 Msun black
holes have re-invigorated the search for PBHs in the 10-100 Msun mass regime.
Unfortunately, individual PBH microlensing events cannot easily be
distinguished from stellar lensing events from photometry alone. However, the
distribution of microlensing timescales (tE, the Einstein radius crossing time)
can be analyzed in a statistical sense using models of the Milky Way with and
without PBHs. While previous works have presented both theoretical models and
observational constrains for PBHs (e.g. Calcino et al. 2018; Niikura et al.
2019), surprisingly, they rarely show the observed quantity — the tE
distribution — for different abundances of PBHs relative to the total dark
matter mass (fPBH). We present a simple calculation of how the tE distribution
changes between models with and without PBHs.

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